adsabs/AstroCLIMB huggingface dataset:
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Image of NuSTAR FPMA for energies >50 keV in Det#1 coordinates. A smoothing Gaussian function has been applied. The stray light contaminates all detectors.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Best fit of the NuSTAR (black) and INTEGRAL-IBIS (red) flux-energy spectrum above 30 keV with model 1 (cutoffpl). Top panel: flux-energy spectrum in units of counts per seconds per keV, both data and model. For the NuSTAR spectrum the dashed line is the cutoff power-law model, the dotted line is the background model, and the solid black line is the total model. Bottom panel: residuals of the best fit.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Top panel: Swift/BAT (black) and MAXI (blue) long-term daily light curves of Cygnus X-1. Bottom panel: hardness ratio as a function of time of Cygnus X-1 computed using MAXI energy bands. In both panels the red dashed lines indicate when the stray light observation was performed and the orange lines indicate NuSTAR pointed observations of Cygnus X-1.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Best fit of the NuSTAR energy spectrum with model 2 (TBabs∗[cutoffpl + relxill]). The hydrogen column density is fixed to 6 × 1021 cm−2. Top panel: flux-energy spectrum in units of counts per seconds per keV, both data and model. The solid line is the total model. The nonsolid lines are the additive components of the model: the dotted line is the background model, the dashed line is the continuum, and the dashed–dotted line is the reflection. Bottom panel: residuals of the best fit.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: Top panel: residuals of model 1 (fit to the overlapping energy range) where we noticed the low energy channels of NuSTAR. Bottom panel: residuals of model 2 (fit to the NuSTAR spectrum) where we added the INTEGRAL-IBIS spectrum and refit only for the cross calibration constant. All the model parameters are tied between NuSTAR and INTEGRAL-IBIS spectra.
Paper: Standard GRB Spectral Models “Misused”?
Authors: Liang Li
Figure caption: The parameter relation of the F–α (left panel), F–E p (middle panel), and α–E p (right panel), as well as the best-fit relations with the 2σ error region.
Paper: NuSTAR Spectral Analysis beyond 79 keV with Stray Light
Authors: G. Mastroserio, B. W. Grefenstette, P. Thalhammer, D. J. K. Buisson, M. C. Brumback, R. M. Ludlam, R. M. T. Connors, J. A. García, V. Grinberg, K. K. Madsen, H. Miyasaka, J. A. Tomsick, J. Wilms
Figure caption: NuSTAR (black) and INTEGRAL (red) light curves during the simultaneous observation.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Comparison of Bayesian fit results for two DM halo models with SPARC data. (A) The leftmost panel shows the SPARC data of 3097 points from 152 galaxies with mass-to-light ratios ϒdisk = 0.5ϒ⊙ for the disk and ϒbulge = 0.7ϒ⊙ for the bulge. Typical uncertainties of the logarithm of accelerations are indicated by error bars at the bottom of the panel. The inset defines the orthogonal residual Δ⊥ from the algebraic MOND relation, i.e., the interpolating function, for a 0 = 1.199× 10−10m s−2 fitted to the outer rotation curves. The other panels show MCMC fit results for the DC14 (Di Cintio et al. 2014a, 2014b), NIHAO (Tollet et al. 2016; Dekel et al. 2017), and FIRE-2 (Lazar et al. 2020) models for hypothetical CDM halos. (B) This panel shows the trend of the medians of orthogonal residuals in the orthogonal bins. DM halo models systematically deviate from the SPARC data, in contrast to the AQUAL model (Chae et al. 2022). Dashed lines are results for a subsample of 111 galaxies without a bulge and with luminosity L < 1011 L ⊙, which reduces the role of BH feedback.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: The inner and outer parts of rotation curves in the acceleration plane. (A) Each SPARC rotation curve shown in Figure 3(a) is separated into the inner rising and outer quasi-flat parts. Data for the two parts are displayed separately and compared with the AQUAL simulated results for the same galaxies. Each panel is in the same format as Figure 3(a). The dashed curve and band indicate the Bayesian fit of Equation (6) to the SPARC data points of the inner or outer part. (B) Histograms show orthogonal residuals from the algebraic MOND relation (red line) for the outer (upper panel) and inner (lower panel) data points. Histograms are fitted with a Gaussian model, and the fitted mean μ (with a bootstrap error) and standard deviation σ are indicated. (C) Solid and dashed lines show the trend of orthogonal residuals in orthogonal bins for the outer and inner parts, respectively. Thick black lines represent the SPARC data while magenta lines represent the AQUAL simulated results. Green lines represent the MCMC fitted results for a subsample of 65 galaxies (Chae et al. 2022) of a good dynamic range that are relatively more massive and larger. Orange lines represent the DC14 results for 111 bulgeless galaxies with L < 1011 L ⊙, which is the most favorable CDM case shown in Figure 3.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Examples of separating a rotation curve into the inner and outer parts. Upper row: three rotation curves of different galaxy type T (as given in Lelli et al. 2016) are shown in the acceleration space based on AQUAL-fitted parameters (Chae et al. 2022). The inset shows the SPARC-reported rotation curves. The inner rising and outer quasi-flat parts were separated visually. A clear inner–outer separation such as these can be done for about 70% of SPARC galaxies (see the text). Lower row: examples in which the outer quasi-flat part is unobserved or ill defined from the SPARC database. For the galaxies without the outer part, AQUAL-fitting (Chae et al. 2022) is not available and thus original SPARC mass models are shown here.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: Comparison of models based on the Bayesian information criterion (BIC). (Left) Comparison between the DC14 halo model and the AQUAL modified gravity model. Only 63 galaxies with inclination ≥30° and outer RCs with good dynamic ranges are shown because the AQUAL modeling was performed with the outer RCs (Chae et al. 2022). For the DC14 model, two cases are considered: fitting the outer RC only, and fitting the entire RC (see the text for details). There are considerable scatters individually. However, from the median there is positive evidence for the AQUAL model consistent with the test by Δ⊥ in Figure 3(b). (Right) Comparing the NIHAO and the FIRE-2 halo models with the DC14 model. The NIHAO model is statistically indistinguishable from the DC14 model. Interestingly, the FIRE-2 model appears not worse than the DC14 model unlike the test based on Δ⊥.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: The distribution of orthogonal residuals Δ⊥ predicted by the DM halo models, as displayed in Figure 3, is compared with that of the SPARC data. From left to right: the DC14 model, the NIHAO model, and the FIRE-2 model in comparison to the SPARC data. The SPARC distribution is represented by the orange histogram while each DM halo predicted distribution is represented by the blue histogram. The DC14 model predicts a 30% larger scatter than the SPARC data while the overall median agrees with the SPARC median. The NIHAO and FIRE-2 models have 20% larger scatters but the overall medians are shifted from the SPARC median.
Paper: Distinguishing Dark Matter, Modified Gravity, and Modified Inertia with the Inner and Outer Parts of Galactic Rotation Curves
Authors: Kyu-Hyun Chae
Figure caption: The upper panel shows the distribution of the inner–outer transition radius R turn for 152 SPARC rotation curves used in this study. The vertical dotted line indicates the median value of 2.6R d where R d is the disk scale radius. The lower panel shows an anticorrelation of R turn/R d with galaxy infrared luminosity. Red dots indicate the outermost radii when the observed RC rises up to the last measured point so that the outer part is unobserved or ill defined.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption:  K-band spectra of the NIR counterparts of the UC H II regions W51e (top), W51e2 (middle), and W51g (bottom). The spectrum of W51e2 with a relatively low signal-to-noise ratio was smoothed by a factor of 3 in an attempt to identify any marginally detected photospheric line. The absence of photospheric features in the spectrum of W51e leads us to classify this source as a MYSO, and W51e2 remains inconclusive. The spectrum of W51g exhibits only photospheric lines typical of late-type stars, inconsistent with the NIR counterpart of a UC H II region (see text for details). Each spectrum was normalized by its continuum, and spectra were not corrected for the heliocentric velocity. The vertical dotted lines indicate typical photospheric lines used to determine the spectral type of massive stars (top) and low-mass stars (bottom), as much as the wavelength of 12CO and 13CO bandheads. Emission lines in the W51e spectrum are artifacts introduced by the sky subtraction step.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: W51e7 velocity channel of He I line. The corresponding wavelength and its relative velocity with respect to its rest wavelength are indicated at the top of each channel. The intensity is scaled in σ units, where σ = rms, and is shown in a blue-to-red divergent scale, as indicated by the color bar at the right. The black contours are placed at 3 n−σ  levels, where n = 0, 1, 2, ...  and the gray contours are placed at −3 n−σ  levels. All velocity channels were corrected for the heliocentric velocity v helio = +6.8 km s−1 and v LSR = +57.4 km s−1.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: Hertzsprung–Russell (H-R) diagram of the UC H II regions studied in this work (black circles), those presented by Figuerêdo et al. (2008) (black triangles), and those presented by Bik et al. (2014) (black squares). The photometric data were corrected using the extinction law from Damineli et al. (2016). In both panels, the solid line represents the ZAMS isochrone and the dotted lines are the main-sequence isochrones as a function of age (left panel) and initial mass (right panel), derived from the evolutionary tracks (including rotation and solar metallicity) presented by Ekström et al. (2012).
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: The distance to W51 Main derived by different works in the literature: n and f represent the near and far kinematic distances, respectively; t indicates that the distance was obtained assuming that the cluster is at the tangent point of the corresponding spiral arm, m indicates a maser distance, and s is for spectrophotometric distance. References: (1) Wilson et al. (1970), (2) Georgelin & Georgelin (1976), (3) Crampton et al. (1978), (4) Downes et al. (1980), (5) Genzel et al. (1982), (6) Imai et al. (2002), (7) Russeil (2003), (8) Kolpak et al. (2003), (9) Sato et al. (2010), and (10) Figuerêdo et al. (2008).
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: Maps (left to right) of the 6 cm continuum emission, NIR continuum, and the continuum-subtracted He I and Brγ features of source W51b2. The white contours indicate the position of the pointlike source and are placed at 10%, 50%, and 90% of the peak intensity of the continuum map. The red square on the radio continuum map represents the NIFS field of view.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: W51e7 velocity channel of the Brγ line (λ 0 = 2.1661 μm). All velocity channels were corrected for the heliocentric velocity v helio = 6.8 km s−1 and v LSR = +57.4 km s−1. See Figure 9 for the full description of the plot.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: Maps (left to right) of the radio 6 cm continuum emission, NIR continuum, and continuum-subtracted He I and Brγ features of source W51e7. The white contours indicate the position of the pointlike source and are placed at 10%, 50%, and 90% of the peak intensity of the continuum map. The red square on the radio continuum map represents the NIFS field of view.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: W51b2 velocity channel of the He I line. All velocity channels were corrected for the heliocentric velocity v helio = +6.54 km s−1 and v LSR = +60.0 km s−1. See Figure 9 for the full description of the plot.
Paper: Near-infrared Spectroscopy of Ultracompact H II Regions in W51A with NIFS/ALTAIR 
Authors: Cassio L. Barbosa, Felipe Navarete, Robert D. Blum, Augusto Damineli, Peter S. Conti
Figure caption: W51b2 velocity channel of the Brγ line. All velocity channels were corrected for the heliocentric velocity v helio = +6.54 km s−1 and v LSR = +60.0 km s−1. See Figure 9 for the full description of the plot.
Paper: One-dimensional Numerical Study on Ignition of the Helium Envelope in Dynamical Accretion during the Double-degenerate Merger
Authors: Kazuya Iwata, Keiichi Maeda
Figure caption: One-dimensional setup shown for the envelope with T base = 2 × 108 K and the mixed-envelope composition (He:C:O = 0.6:0.2:0.2 in the mass fractions). The envelope region is colored yellow and the region with the mass accretion source is colored blue.
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Constraints on Ωm and w in the wCDM model at high redshift z > 1.4 only with 140 GRBs (left panel), and 98 GRBs (right panel). H 0 is set to be 70 km s−1 Mpc−1.
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Joint constraints on parameters of Ω m  and h in the ΛCDM model at high redshift z > 1.4 with 140 GRBs + 31 OHD (left panel), and 98 GRBs + 31 OHD (right panel).
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Joint constraints on parameters of Ωm, h and w in the wCDM model at high redshift z > 1.4 with 140 GRBs + 31 OHD (left panel), and 98 GRBs + 31 OHD (right panel).
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Simultaneous fitting parameters of Ω m , h, a, b, σ int, and w in the wCDM model with A219 GRBs + 31 OHD (left panel), and A118 GRBs + 31 OHD (right panel).
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Simultaneous fitting parameters of Ω m , h, a, b, and σ int in the ΛCDM model with A219 GRBs + 31 OHD (left panel), and A118 GRBs + 31 OHD (right panel).
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: The spectroscopic (black curve) and photometric (filled squares in cyan) data of J1605+4743 plotted in the rest frame of the quasar, in comparison with its counterpart, J1105+0457 (green: the spectrum; orange: the photometry). The original photometric data of J1105+0457 are shown as crosses in orange. The orange empty squares are these data normalized to the flux level of J1605+4743 at the WISE W4 band by multiplying a factor of 0.78, after k-correction. The spectrum of J1105+0457 is also scaled by a factor of 0.78, and shown as the green curve. The Hα emission line is prominent in the spectra of both quasars, while [O II] is only present in the spectrum of J1605+4743 (as labeled above the data in the plot). Also labeled are Fe II and Mg II narrow absorption lines that appear only in J1605+4743. The SEDs of the two quasars show little difference at λ rest ≳ 10,000 Å, whereas the two SEDs begin to show significant differences at λ rest ≲ 10,000 Å. This difference increases dramatically at shorter wavelengths, and reaches its maximum at λ rest ∼ 2175 Å, as indicated by the red arrow. The insert panel shows the observed radio spectrum of J1605+4743 (empty squares), overlaid with the best-fit result of a power law (dashed line).
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: In the left panels, the optical-NIR spectra of four unusual quasars (black lines) are compared with that of J1605+4743 (blue lines), and the average template (dark green lines) of J1105+0457, PG1407+265 and PHL1811. Extinction curves of these quasars are then derived (black lines in the right panels). These extinction curves can be approximated reasonably well using a second-order polynomial (gray dashed lines), just like the underlying extinction of J1605+4743(blue lines), but no significant 2175 Å bump is found in these targets. Compared to the averaged extinction curve of MW sight lines (light green lines), these unusual quasars and J1605+4743 have relatively steeper extinction slope, suggesting that dust grains are mainly of small sizes in the sight lines of these quasars.
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: (a) Comparison of the extinction curve of J1605+4743 with Milky Way sightlines with their extinction curves. The extinction curve of J1605+4743 can be best approximated by HD 210121 (green line). The envelope of the well-matched MW sightlines is shown in orange. (b) Comparison of the extinction curve of J1605+4743 with a theoretical dust model (red curve), which has components of carbonaceous (dashed blue) and astronomical silicate (dotted purple) grains.
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: Selected emission lines of J1605+4743 plotted in their common velocity space, after removal of the best-fit model of the continuum and pseudo-continuum of Fe II emission. In panel (a), Hβ and Hγ are scaled by a proper factor (as indicated by the color-coded legends) for a comparison with Hα. Note the close resemblance of the three Balmer lines, which are only slightly broader than [O II]. Data of [O II], Hα, [O III], and Mg II are compared with the best-fit models in panels (b), (c), (d), and (e), respectively (see the text in Section 5 for details).
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: Calculated extinction curve overlaid with models. Black curve is the ratio of the spectrum of J1605+4743 to the scaled J1105+0457 as a function of x = λ −1. The cyan filled squares are obtained by the photometric ratio of these two quasars (see Section 3 for details). These calculations can be well reproduced by the combination (green) of a Drude profile (orange) characterizing the 2175 Å bump and a linear underlying extinction (blue). Beside the noisy ends of the curve, the spikes and troughs at 2 ≲ x ≲ 4.5 are caused by absorption and emission lines as labeled in the plot.
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: In the top panels sequenced as (1)–(3) from left to right, the two-epoch SDSS/BOSS spectra and the P200/DBSP spectrum are individually plotted, comparing with the average of the three spectra and the photometric data of J1605+4743. In the left panels sequenced as (a)–(c) from top to bottom, the three NLS1-WLQ hybrid templates are compared with the quasar composite. The extinction curves are then derived for each spectrum of J1605+4743 relative to different templates in panel (a1)–(c3) in the right-bottom panels. The derived extinction curves are compared with their best-fit results (green lines), a combination of the underlying extinction (blue line) and the 2175 Å extinction bump (orange line).